On a Babcock-Leightom dynamo model with a thin, deep seated generating layer for the toroidal field.
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**Session 92 -- Solar Active Regions and Solar Wind**
*Oral presentation, Wednesday, 11, 1995, 10:00am - 11:30am*

## [92.01] On a Babcock-Leightom dynamo model with a thin, deep seated generating layer for the toroidal field.

*Bernard R. Durney (University of Arizona and Zetetic Institute)*

The following dynamo model will be discussed and hopefully
numerical results will be presented.
Let $A$ be the vector potential for the axisymmetric poloidal
field, and $B,$ the toroidal field. $B$ is generated by a shear
in the angular velocity acting on $A$ in a thin layer located in
the lower solar convection zone. If in this layer $B$ exceeds a
critical value for a certain value of theta (the polar
angle), eruption occurs. The flux tube is assumed to rise radially
and to surface as a magnetic ring doublet. The rates of eruption of
the ensemble of these doublets constitute the source term of the
equation for $\partial A / \partial t$ that regenerates the poloidal
field. The poloidal field generated in the solar surface layers reaches
the lower solar convection by transport due to meridional motions and
by diffusion. The meridional motions being considered are the
superposition of a one-cell velocity field that rises at the equator
and sinks at the poles and of a two-cell motion that rises at the
equator and poles and sinks at mid latitudes. Meridional motions of
this type have a strong theoretical and observational support.

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